J2345-0449

Last updated
J2345-0449
SDSS image of J2345-0449.jpg
SDSS image of J2345-0449
Observation data (J2000 epoch)
Constellation Aquarius
Right ascension 23h 45m 32.70s
Declination −04° 49′ 25.4″
Redshift 0.075566
Heliocentric radial velocity 22,654 km/s
Distance 947 Mly (290.3 Mpc)
Apparent magnitude  (V)0.086
Apparent magnitude  (B)0.113
Surface brightness 16.19
Characteristics
Apparent size  (V)0.62' x 0.31'
Notable featuresOne of the most massive spiral galaxies containing a radio jet
Other designations
PGC 1052974, GRS J2345-0449, 2MASX J23453268-0449256, 6dF J2345327-044925

J2345-0449 or 2MASX J23453268-0449256, is a spiral galaxy located 947 million light-years in the constellation of Aquarius. [1] It contains an active galactic nucleus and is classified as a radio galaxy, containing relativistic jets that are projected out from its spiral host by ~1.6 Mpc, making these jets the largest and rarest known. [2] [3] It was discovered in 2014 by amateur astronomers, making it the third spiral DRAGN after ESO 0313-192 and Speca. [2]

Contents

Physical Properties

Mentioned as a megaparsec-scale object at redshift 0.0757, [4] J2345-0449 is one of the massive spiral galaxies found in the universe. [5] [6] It is also one of the largest radio sources discovered since the galaxy exhibits two sets of radio lobes found in near alignment and spanning a width of ∼387.2 kpc (∼452) and ∼1.63 Mpc (∼191). [2] According to Very Large Array 6 cm imaging, the inner radio lobes are categorized either Fanaroff-Riley Class I or FR II morphology. [7]

J2345-0449 contains a fast rotation speed of Vrot = 371/sin (i) = 429 ± 30 km s−1 that is r ≥ 10 kpc away from its galactic center. [8] It has a mass of Mstellar = 4 × 1011 M⊙ and a surrounding ring of molecular gas measured 24 kpc wide in diameter. The galaxy has a star formation rate with a surface density measured to be ΣSFR = 1.8 × 10−3 M⊙ yr−1 kpc−2. [9] However it has a low factor between 30 and 70 as expected according to the Kennicutt-Schmidt law. [10]

Black hole mass of J2345-0449

The black hole mass estimation is challenging since J2345-0449 has no classic bulge structure. According to Bagchi, the black hole has a mass of 2.5 ± 0.5 × 108 M⊙. Further observations shows it has a mass of 1.4× 109 M⊙ when calculating the MBH–σ relation proposed by Gültekin. [11] However, according to researchers obtaining the M–σ relation from McConnell & Ma, [12] the actual mass of J2345-0449 is 5 × 109 M⊙. [8]

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that this luminosity is not produced by the stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

<span class="mw-page-title-main">MS 0735.6+7421</span> Galaxy cluster in the constellation Camelopardalis

MS 0735.6+7421 is a galaxy cluster located in the constellation Camelopardalis, approximately 2.6 billion light-years away. It is notable as the location of one of the largest central galactic black holes in the known universe, which has also apparently produced one of the most powerful active galactic nucleus eruptions discovered.

<span class="mw-page-title-main">Swift J1644+57</span> Tidal disruption event in the constellation Draco

Swift J164449.3+573451, initially referred to as GRB 110328A, and sometimes abbreviated to Sw J1644+57, was a tidal disruption event (TDE), the destruction of a star by a supermassive black hole. It was first detected by the Swift Gamma-Ray Burst Mission on March 28, 2011. The event occurred in the center of a small galaxy in the Draco constellation, about 3.8 billion light-years away. It was the first confirmed jetted tidal disruption event and is the most luminous and energetic TDE recorded.

<span class="mw-page-title-main">RX J1532.9+3021</span> Galaxy cluster in Corona Borealis

RX J1532.9+3021 is a galaxy cluster located in the constellation of Corona Borealis. It has a velocity of 103,539 ± 8 kilometers per second, equivalent to a Hubble distance of 1,527.1 ± 106.9 megaparsecs or 3.9 billion light years. It is classfied one of the massive and strongest X-ray bright cool clusters in the universe at redshift z = 0.362. The luminosity of the cluster is estimated to be 6 x 1045 ergs-1. According to a study published in 2013, a mini radio halo is seen surrounding the cluster.

<span class="mw-page-title-main">NGC 3862</span> Galaxy in the constellation Leo

NGC 3862 is an elliptical galaxy located 300 million light-years away in the constellation Leo. Discovered by astronomer William Herschel on April 27, 1785, NGC 3862 is an outlying member of the Leo Cluster.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 4061</span> Galaxy in the constellation Coma Berenices

NGC 4061 is an elliptical galaxy located 310 light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 27, 1785. It was rediscovered by John Herschel on April 29, 1832. It is listed both as NGC 4061 and NGC 4055. NGC 4061 is a member of the NGC 4065 Group and forms an interacting pair with its companion, NGC 4065 as evidenced by distortions in their optical isophotes.

<span class="mw-page-title-main">NGC 4294</span> Galaxy in the constellation Virgo

NGC 4294 is a barred spiral galaxy with flocculent spiral arms located about 55 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">III Zw 2</span> Seyfert galaxy in the constellation Pisces

III Zw 2 is a Seyfert 1 galaxy located in the Pisces constellation. It has a redshift of 0.089 and is notable as the first of its kind to exhibit a superluminal jet.

<span class="mw-page-title-main">4C +29.30</span> Galaxy in the constellation Cancer

4C +29.30 is an elliptical galaxy located in Cancer constellation. Its redshift is 0.064840 which corresponds to a light travel time of 850 million light-years from Earth. It is a wide-angled tailed radio galaxy (WAT) and a Seyfert galaxy.

<span class="mw-page-title-main">MRC 0406-244</span> Radio galaxy producing an astrophysical jet in the constellation of Eridanus

MRC 0406-244 also known as TN J0408-2418, is a radio galaxy producing an astrophysical jet, located in the constellation of Eridanus. At its redshift of 2.44, it is roughly ten billion light years from Earth.

<span class="mw-page-title-main">MRC 2011-298</span> Brightest cluster galaxy in the constellation Sagittarius

MRC 2011-298 is an elliptical galaxy with an active galactic nucleus, located in the constellation of Sagittarius. It is located 2.1 billion light-years away from Earth. MRC 2011-298 is the brightest cluster galaxy in the galaxy cluster, Abell 3670 and classfied as a dumbbell galaxy, an optical system with two galactic nuclei separated by 7″, corresponding to ≃17 kpc according to the adopted cosmology, with similar magnitude and a common stellar halo. The galaxy is known to have an ellipticity of ε = 0.28 and a position angle of PA  =  24° that is measured from north to east.

<span class="mw-page-title-main">4C +72.26</span> Radio galaxy in the constellation Draco

4C +72.26 known as NAME TX J1908+7220, is a radio galaxy located in the constellation Draco. At the redshift of 3.53, the galaxy is located roughly 11.5 billion light-years from Earth.

<span class="mw-page-title-main">NGC 4325</span> Galaxy

NGC 4325 is an elliptical galaxy located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on April 15, 1865, who described it as "vF, vS, iR, nf of 2". Despite being listed in the Virgo Cluster catalog as VCC 616, it is not a member of the Virgo Cluster but instead a background galaxy.

<span class="mw-page-title-main">NGC 6051</span> Galaxy in the constellation of Serpens

NGC 6051 is a giant elliptical galaxy located in the constellation of Serpens. The galaxy lies 453 million light-years from Earth, which means given its apparent dimensions, the galaxy is around 250,000 light-years across. It is the brightest cluster galaxy inside a relaxed poor cluster called AWM 4, a fossil system, making up of at least 30 galaxy members.

<span class="mw-page-title-main">SDSS J0849+1114</span> Trio of interacting galaxies in the constellation Cancer

SDSS J0849+1114 is a late-stage galaxy merger forming from a trio of galaxies located in the constellation of Cancer. At the redshift of 0.077, they are located 1.06 billion light-years from Earth. First discovered as a triple active galactic nucleus (AGN) candidate in a Sloan Digital Sky Survey study published in 2011, they received significant attention when astronomers discovered it harbors three supermassive black holes in its center.

<span class="mw-page-title-main">J1000+1242</span> Type 2 quasar located in the constellation Leo

J1000+1242 known as SDSS J1000+1242 or J1000+12 is a radio-quiet type-2 quasar, located in the constellation Leo. It is located 2 billion light years from Earth and is classified as a Seyfert galaxy.

References

  1. ↑ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-07-16.
  2. 1 2 3 Bagchi, Joydeep; Vivek, M.; Vikram, Vinu; Hota, Ananda; Biju, K. G.; Sirothia, S. K.; Srianand, Raghunathan; Gopal-Krishna; Jacob, Joe (2014-06-05). "Megaparsec Relativistic Jets Launched from an Accreting Supermassive Black Hole in an Extreme Spiral Galaxy". The Astrophysical Journal. 788 (2): 174. arXiv: 1404.6889 . doi:10.1088/0004-637x/788/2/174. ISSN   0004-637X.
  3. ↑ Walker, Stephen (2013-09-01). "Detecting the hot gaseous halo around an extremely massive and relativistic jet launching spiral galaxy". Chandra Proposal: 3824. Bibcode:2013cxo..prop.3824W.
  4. ↑ Machalski, J.; Koziel-Wierzbowska, D.; Jamrozy, M. (2007-10-24), Giant Radio Galaxies as a probe of the cosmological evolution of the IGM, I. Preliminary deep detections and low-resolution spectroscopy with the SALT, arXiv: 0710.4512
  5. ↑ Posti, Lorenzo; Fraternali, Filippo; Marasco, Antonino (2019-06-01). "Peak star formation efficiency and no missing baryons in massive spirals". Astronomy and Astrophysics. 626: A56. arXiv: 1812.05099 . Bibcode:2019A&A...626A..56P. doi:10.1051/0004-6361/201935553. ISSN   0004-6361.
  6. ↑ Bagchi, Joydeep; Ray, Shankar; Dhiwar, Suraj; Dabhade, Pratik; Barth, Aaron; Ho, Luis C.; Mirakhor, Mohammad S.; Walker, Stephen A.; Nesvadba, Nicole (2024-05-03), Unveiling the Bulge-Disc Structure, AGN Feedback, and Baryon Landscape in a Massive Spiral Galaxy with Mpc-Scale Radio Jets, arXiv: 2405.01910 , retrieved 2024-07-16
  7. ↑ Parma, P. (1982), "Westerbork Observations of Low Luminosity Radio Sources", Extragalactic Radio Sources, Dordrecht: Springer Netherlands, pp. 193–194, doi:10.1007/978-94-009-7781-5_55, ISBN   978-94-009-7783-9 , retrieved 2024-07-16
  8. 1 2 Walker, S. A.; Bagchi, J.; Fabian, A. C. (2015-04-09). "A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy". Monthly Notices of the Royal Astronomical Society. 449 (4): 3527–3534. arXiv: 1411.1930 . doi: 10.1093/mnras/stv616 . ISSN   0035-8711.
  9. ↑ Nesvadba, N. P. H.; Wagner, A. Y.; Mukherjee, D.; Mandal, A.; Janssen, R. M. J.; Zovaro, H.; Neumayer, N.; Bagchi, J.; Bicknell, G. (2021-10-01). "Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo". Astronomy & Astrophysics. 654: A8. arXiv: 2103.12816 . doi:10.1051/0004-6361/202140544. ISSN   0004-6361.
  10. ↑ Drevet Mulard, M.; Nesvadba, N. P. H.; Meenakshi, M.; Mukherjee, D.; Wagner, A.; Bicknell, G.; Neumayer, N.; Combes, F.; Zovaro, H.; Janssen, R. M. J.; Bagchi, J.; Dabhade, P.; Prunet, S. (2023-08-01). "Star formation in a massive spiral galaxy with a radio-AGN". Astronomy and Astrophysics. 676: A35. Bibcode:2023A&A...676A..35D. doi:10.1051/0004-6361/202245173. ISSN   0004-6361.
  11. ↑ Gültekin, Kayhan; Cackett, Edward M.; Miller, Jon M.; Di Matteo, Tiziana; Markoff, Sera; Richstone, Douglas O. (2009-11-01). "The Fundamental Plane of Accretion onto Black Holes with Dynamical Masses". The Astrophysical Journal. 706 (1): 404–416. arXiv: 0906.3285 . Bibcode:2009ApJ...706..404G. doi:10.1088/0004-637X/706/1/404. ISSN   0004-637X.
  12. ↑ McConnell, Nicholas J.; Ma, Chung-Pei (2013-02-01). "Revisiting the Scaling Relations of Black Hole Masses and Host Galaxy Properties". The Astrophysical Journal. 764 (2): 184. arXiv: 1211.2816 . Bibcode:2013ApJ...764..184M. doi:10.1088/0004-637X/764/2/184. ISSN   0004-637X.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.